Contact Binaries with Additional Components. I. The Extant Data

Pribulla, T.; Ruciński, S. M.

doi:10.1086/503871

Cited by 292 publications

(240 citation statements)

References 73 publications

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“…Some of them are eclipsing binaries with a pulsating component, and some semi-regular variables with unknown short-term variations or some pulsating ellipsoidal variables (Derekas et al 2006;Nie, Zhang, & Jiang 2010;Faigler & Mazeh 2011;Faigler et al 2012). In several studies, V1464 Aql was classified as a spectroscopic binary system, RR Lyr (RRc), an eclipsing binary, possibly contact (EC) or semi-detached system (ESD) (Duerbeck 1997;Pourbaix et al 2004;Pribulla & Rucinski 2006; PASA, 30, e016 (2013) doi:10.1017/pasa.2012.016 Aerts et al (2002). c Henry et al (2004).…”

Section: Resultsmentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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Taking into account the results obtained from the models and analyses of the BVRI light curves, we discuss the nature of V1464 Aql. The analyses indicated that the mass ratio of the system is q = 0.71 ± 0.02, while the inclination of the system (i) is 38°.45 ± 0°.22. Taking the primary component's temperature as 7 420 ± 192 K, we found that the temperature of the secondary is 6 232 ± 161 K. The mass of the primary component was found to be 1.74 ± 0.05 M ࣻ , while it is 1.23 ± 0.01 M ࣻ for the secondary. The primary component's radius was found to be 2.10 ± 0.05 R ࣻ , while it was found as 1.80 ± 0.01 R ࣻ for the secondary. Revealing that the system should not exhibit any eclipses, we demonstrated that the main variation with large amplitude should be caused due to the ellipsoidal effect. Indeed, the Fourier analysis also supported the result. For the first time in the literature, we revealed that the primary component is a δ Scuti star. The period of pulsation was found to be 58.482 ± 0.002, 58.482 ± 0.001, 60.966 ± 0.002, and 60.964 ± 0.003 min in BVRI bands, respectively. We plotted V1464 Aql in the log(P orb )-log (P pulse ) plane. Using more than 160 binaries, whose one or both components are pulsating, we derived a new linear fit in the log (P orb )-log (P pulse ) plane for each type of binary. Using the linear fit of each group, we obtained new calibrations between log (P orb ) and log (P pulse ) for different types of pulsating stars. In addition, a calibration has been obtained for the first time for the pulsating stars with spectral types O and B. V1464 Aql seems to be located near the other ellipsoidal and close binaries. Thus, we listed V1464 Aql as a new candidate for the ellipsoidal variables with a δ Scuti component.

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Section: Resultsmentioning

confidence: 99%

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Dal

Sipahi

2013

Publ. Astron. Soc. Aust.

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“…Yang & Liu (2003) considered both mass exchange and mass loss mechanisms that could cause the observed decrease in the period but found that the cyclic variation superimposed on the decreasing trend was quasi-periodic; hence, it could only be attributed to magnetic activity. Pribulla & Rucinski (2006) and Rucinski et al (2007) did not detect the signature of a third body in their studies dedicated to detecting faint third bodies in contact binary systems. In addition, broadening functions constructed for radial velocity analysis by Pribulla et al (2009a) did not show any evidence of a third companion in the system.…”

Section: Rw Commentioning

confidence: 96%

Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

Djurašević

Yılmaz

Baştürk

et al. 2010

A&A

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Aims. We analyze new multicolor light curves and recently published radial velocity curves for close binaries QX And, RW Com, MR Del, and BD +07 • 3142 to determine the physical parameters of the components. Methods. The light curves are analyzed using a binary star model based on Roche geometry to fit the photometric observations. Spectroscopic parameters, such as the mass ratios and spectral types, were taken from recent spectroscopic studies of the systems in question. Results. Our findings provide consistent and reliable sets of stellar parameters for the four studied binary systems. Of particular interest is the BD +07 • 3142 system, since this is the first analysis of its light curves. We find that it is an overcontact binary of W UMa type and W subtype, and that each component has a large cool spot in the polar region. QX And is an A subtype, and RW Com a W subtype W UMa binary, and in both systems we find a bright spot in the neck region between the components. MR Del is a detached binary with a complex light curve that we could model with two cool spots on the hotter component.

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“…Tokovinin & Smekhov (2002) have noted that periods above ∼ 10 days are rarer (relative to shorter periods) among the inner binaries of triples than in the population as a whole, and possibly this is accounted for by the combination of Kozai cycles and tidal friction (KCTF). Pribulla & Rucinski (2006) have noted that as many as 42% of contact binaries appear to be in triples (and arguably 59% in a more thoroughly examined subsample), and it could be that KCTF has contributed to this; although we probably need the additional influence of magnetic braking to drive fairly close low-mass binaries generated by KCTF to contact on a timscale of < ∼ 10 9 .…”

Section: Discussionmentioning

confidence: 96%

The Incidence of Multiplicity Among Bright Stellar Systems

2006

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Abstract.We consider the multiplicity of stellar systems with (combined) magnitude brighter than 6.00 in Hipparcos magnitudes. We identify 4555 such bright systems, and the frequencies of multiplicities 1, 2, . . . , 7 are found to be 2722, 1412, 299, 86, 22, 12 and 2. We also consider the distributions of periods of orbits and sub-orbits. For the even more restricted set of 474 systems with VH 4.00 the proportions of higher multiples up to sextuple are progressively larger, suggesting incompleteness in even the relatively well-studied larger sample.We construct a Monte-Carlo algorithm that will generate systems with roughly the observed multiplicities and orbital parameters, taking account of selection effects.

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Contact Binaries with Additional Components. I. The Extant Data

Cited by 292 publications

References 73 publications

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

The Nature of V1464 Aql: A New Ellipsoidal Variable with a δ Scuti Component

Physical parameters of close binaries QX Andromedae, RW Comae Berenices, MR Delphini, and BD +07° 3142

The Incidence of Multiplicity Among Bright Stellar Systems

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